2 Chirped pulse juxtaposed with beam amplification

High-saturation fluence gain materials, for example Nd:glass and Yb:glass, require a highly stretched temporal pulse to extract the full stored energy while avoiding optical damage from B-integral accumulation leading to small-scale self-focusing. Small-scale self-focusing is initiated by the high-frequency spatial noise content on the beam, which can be reduced by a spatial filter. Extensive experimental work on high-energy Nd:glass laser systems has suggested a delta B-integral, the B-integral accumulated between passes through a spatial filter, a limit of 3 and a cumulative B-integral, total B-integral accumulated, of 5–6^[ Reference Simmons, Hunt and Warren ^{60 –} Reference Van Wonterghem, Murray, Campbell, Speck, Barker, Smith, Browning and Behrendt ^{62 ]}. The greater the amount of stored energy in the amplifier, the longer the stretched pulse duration required – this is one of the primary reasons why high-energy, Nd:glass laser systems operate at a small portion, around 10%, of their total stored energy. The NIF has shown that a stretched pulse of 23 ns is able to safely extract the full 26 kJ of stored energy in a single amplifier beamline^[ Reference Van Wonterghem, Burkhart, Haynam, Manes, Marshall, Murray, Spaeth, Speck, Sutton and Wegner ^{50 ]}. However, as the stretched pulse duration extends into the nanosecond regime a practical problem emerges: the gratings must be large enough to handle a nanosecond-scale delay between the red and blue components of the spectrum. A delay of 1 ns equates to approximately 30 cm of path difference, and when projected onto a grating at its operating angle-of-incidence (AOI) requires meter-scale grating apertures. Furthermore, large-area beams, as found on high-energy Nd:glass lasers, are very inefficient in their use of the grating aperture for temporal compression as the maximum normal separation of a grating pair, and hence the maximum negative group delay dispersion (GDD) induced on the pulse is limited, in part, by the spatial beam width. In a previous publication we detailed how to enhance the temporal compression efficiency of a grating pair by spatially chirping the input beam to allow for greater grating separation^[ Reference Chesnut and Barty ^{63 ]}. This chirped-beam grating pair led to the design of the six-grating compressor and is one of the fundamental components of CPJBA^[ Reference Barty ^{34 ,} Reference Chesnut and Barty ^{63 ]}. In a typical grating pair compressor, the maximum normal grating separation is given by the following:

(1) $$\begin{align}{L}_\mathrm{max}=\frac{G-\frac{w}{\cos \left(\gamma \right)}}{\tan \left({\theta}_\mathrm{r}\right)-\tan \left({\theta}_\mathrm{b}\right)},\end{align}$$

where $G$ is the width of the second grating, $w$ is the input beam width, $\gamma$ is the AOI on the first grating and ${\theta}_\mathrm{r}$ and ${\theta}_\mathrm{b}$ are the diffracted angles of the red-most and blue-most components of the spectrum, respectively, as determined by the grating equation^[ Reference Chesnut and Barty ^{63 ]}. Figure 2 graphically demonstrates the effect that the input beam width has on the maximum grating separation, where a smaller beam enables a larger grating separation before clipping.

In developing the ARC PW laser, the Lawrence Livermore National Laboratory (LLNL) produced high-efficiency, high-damage-threshold multi-layer dielectric (MLD) gratings with a groove density of 1780 lines/mm and AOI of 76.5 degrees^[ Reference Britten, Molander, Komashko and Barty ^{53 ]}. Current ARC gratings are approximately 0.9-m wide^[ Reference Barty, Key, Britten, Beach, Beer, Brown, Bryan, Caird, Carlson, Crane, Dawson, Erlandson, Fittinghoff, Hermann, Hoaglan, Iyer, Jones, Jovanovic, Komashko, Landen, Liao, Molander, Mitchell, Moses, Nielsen, Nguyen, Nissen, Payne, Pennington, Risinger, Rushford, Skulina, Spaeth, Stuart, Tietbohl and Wattellier ^{64 ]}, but it is believed the grating manufacturing equipment, used by the Plymouth Grating Laboratory and LLNL, can be scaled up to produce 2-m-wide gratings^[ Reference Erdogan ^{65 ]}. Horiba France has produced the approximately 0.575-m × 1.015-m gratings currently used on the ELI-NP HPLS compressor^[ Reference Lureau, Matras, Chalus, Derycke, Morbieu, Radier, Casagrande, Laux, Ricaud, Rey, Pellegrina, Richard, Boudjemaa, Simon-Boisson, Baleanu, Banici, Gradinariu, Caldararu, Boisdeffre, Ghenuche, Naziru, Kolliopoulos, Neagu, Dabu, Dancus and Ursescu ^{17 ]} and 0.66-m × 1.41-m gratings that have undergone experimental demonstration at SIOM^[ Reference Han, Li, Zhang, Kong, Cao, Jin, Leng, Li and Shao ^{66 ]}. Given the ARC grating design, with a maximum aperture of 2 m, and a 37-cm beam width, as is commonly found on large-aperture Nd:glass lasers^[ Reference Neauport, Airiau, Beck, Belon, Bordenave, Bouillet, Chanal, Chappuis, Coic, Courchinoux, Denis, Gaudfrin, Gaudfrin, Gendeau, Heymans, Julien, Lacombe, Lamy, Lebeaux, Luttmann, Modelin, Perrin, Ribeyre, Rouyer, Tournemenne, Valla and Vermersch ^{47 ,} Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}, a standard four-grating compressor can compress, at maximum, a 3.34-ns stretched pulse down to a 100-fs FTL.

Figure 2

Illustration of how the grating pair is limited by the angular dispersion of the red-most and blue-most frequency components along with the aperture size of the second grating.

Figure 3

Illustration of a chirped-beam grating pair interacting with a spatially chirped-beam pulse with a $\chi$ of two.

The compressive effect of a maximum-aperture-limited grating pair can be extended by employing spatial chirp on the input beam^[ Reference Chesnut and Barty ^{63 ]}. Spatial chirp is defined as a varying spatial location, transverse to the direction of propagation, of the frequency components in a laser pulse^[ Reference Gu, Akturk and Trebino ^{68 ]}. Spatial chirp can be conveniently described by the spatial chirp parameter, $\chi$ , which normalizes the spatial chirp to the beam size. Here, $\chi$ represents the total beam width expansion factor due to spatial chirp; a $\chi$ of two represents a beam whose red-most and blue-most components (i.e., the spectral cutoff frequencies that experience zero clipping on the grating aperture) have been separated a transverse distance equal to the initial beam width. Generally, spatial chirp is created by optics that induce angular dispersion. For example, in Figure 2 the pulse enters the first grating with all the frequency components overlapped in space; the first grating imparts angular dispersion to the pulse causing the frequency components to spatially separate; the second grating removes the angular dispersion yet the frequency components remain spatially separated. Consider further separating the grating pair until the input beam has doubled from the original full-width due to the spatial chirp of the spectral components. Now, as illustrated in Figure 3, the input beam has a spatial chirp parameter of two (i.e., the red and blue components of the pulse have been separated transversely in space by a distance equivalent to the original beam width) and the optical path length difference of the spectral components between the grating pair is increased. We refer to this simultaneous spatial and temporal chirp as a chirped-beam pulse. With this, the maximum normal grating separation becomes^[ Reference Chesnut and Barty ^{63 ]}

(2) $$\begin{align}{L}_\mathrm{max}=\frac{G-\frac{w\left(2-\chi \right)}{\cos \left(\gamma \right)}}{\tan \left({\theta}_\mathrm{r}\right)-\tan \left({\theta}_\mathrm{b}\right)}.\end{align}$$

For the ARC grating design, a full-width beam of 37 cm and a pulse with spectral content ranging from 1040 to 1070 nm, this chirped-beam pulse grating pair generates 425% more negative GDD than the traditional grating pair^[ Reference Chesnut and Barty ^{63 ]}.

Figure 4

Schematic of the six-grating compressor for CPJBA designed to compress a 37-cm × 37-cm aperture simultaneously spatially and temporally chirped 20-ns pulse down to an 18.5-cm × 37-cm aperture 100-fs Fourier transform-limited pulse^[ Reference Chesnut and Barty ^{63 ]}.

Figure 5

Flow chart diagram of the Nexawatt laser.

CPJBA enables highly efficient temporal compression of large-aperture beams with a novel six-grating compressor, shown in Figure 4. Here, two chirped-beam pulse grating pairs (G1-G2 and G3-G4) perform a majority of the temporal compression but leave the spatial chirp unchanged. The chirped-beam pulse then enters a final grating pair that removes the spatial chirp and performs the remaining amount of temporal compression. In this way, one can compress a 20-ns stretched pulse down to its 100-fs FTL using ARC gratings with a maximum aperture of 2 m. As mentioned previously, the final grating has a finite damage threshold of approximately 1 J/cm² at 100 fs^[ Reference Britten ^{54 ,} Reference Alessi, Carr, Hackel, Negres, Stanion, Fair, Cross, Nissen, Luthi, Guss, Britten, Gourdin and Haefner ^{55 ]} and cannot handle the full power of the compressed pulse. Instead, through a careful arrangement of beam splitters, the chirped-beam pulse is split into multiple identical beamlet copies prior to total temporal compression by as many final grating pairs – this effectively increases the aperture of the final grating, reducing the fluence seen on the final optic. Since the beamlets all originate from the same amplifier there is a single wavefront distortion to correct for, and all beamlets will be identical to the extent that the beam splitters and final gratings can be made identical. To accomplish this compression factor with a standard four-grating Tracey compressor, the ARC grating design would require a grating aperture of 5.4 m (height) × 1.6 m (wide) for gratings 1 and 4, and 5.4 m (height) × 6.14 m (wide) for gratings 2 and 3. Supposing a maximum grating aperture of 0.5 m (height) × 2 m (wide), to drop the fluence below the 1-J/cm² damage limit the tiled grating approach would need 11 × 1 tiled gratings for gratings 1 and 4 and 11 × 4 tiled gratings for gratings 2 and 3 – a total of 110, 2-m wide gratings. Each of these gratings has 5 degrees-of-freedom that require nm-scale alignment precision to properly maintain the pulse structure^[ Reference Blasiak and Zheleznyak ^{35 –} Reference Yang, Qi, Mi, Zhang, Yu, Yu, Li and Yang ^{37 ]}. In contrast, the CPJBA six-grating compressor involves only two, 2-m aperture gratings as most of the gratings are 1.6 or 0.8-m wide, and it has lower complexity alignment and does not require masking the beam.

3 Nexawatt system overview

The Nexawatt (NIF Exawatt) system is based on a single aperture of a modified NIF beamline that incorporates an OPCPA front-end and Nd:mixed-glass main amplifiers (MAs), similar to the Texas Petawatt and ELI-Aton lasers^[ Reference Rus, Bakule, Kramer, Naylon, Thoma, Green, Antipenkov, Fibrich, Novák, Batysta, Mazanec, Drouin, Kasl, Baše, Peceli, Koubíková, Trojek, Boge, Lagron, Weiss, Hřebček, Hříbek, Durák, Polan, Košelja, Korn, Horáček, Horáček, Himmel, Havlíček, Honsa, Korouš, Laub, Haefner, Bayramian, Spinka, Marshall, Johnson, Telford, Horner, Deri, Metzger, Schultze, Mason, Ertel, Lintern, Greenhalgh, Edwards, Hernandez-Gomez, Collier, Gaul, Martinez, Frederickson, Hammond, Malato, White and Houžvička ^{25 ,} Reference Gaul, Martinez, Blakeney, Jochmann, Ringuette, Hammond, Borger, Escamilla, Douglas, Henderson, Dyer, Erlandson, Cross, Caird, Ebbers and Ditmire ^{69 ]}, that utilizes the CPJBA scheme to potentially extend its peak power into the exawatt regime. Nd:glass amplifiers have been traditionally considered ‘narrow-bandwidth’ amplification mediums; however, when the amplifier is composed of mixed substrate glass it can support a much broader spectrum enabling high-energy, short-pulse amplification. In 2007 Hays et al. ^[ Reference Hays, Gaul, Martinez and Ditmire ^{51 ]} showed in a numerical study that an initial amplification stage of K-824 Nd:silicate glass slabs followed by a second amplifier composed of APG-1 Nd:phosphate glass slabs can have with total gain 104 while supporting an amplified bandwidth capable of producing approximately 100-fs FTL pulses. Using a 20-ns chirped-beam pulse to extract the full energy from a NIF-like beamline composed of Nd:mixed glass could potentially result in, after diffraction losses from a CPJBA six-grating compressor, approximately 20 kJ in a 100-fs FTL pulse – a 0.2-EW peak-power laser. The general architecture of the full Nexawatt energetics chain is based on the conceptual schematic presented by Hays et al. ^[ Reference Hays, Gaul, Martinez and Ditmire ^{51 ]}.

A top-level flow chart of the Nexawatt system is shown in Figure 5. The pulse originates from a Ti:sapphire mode-locked oscillator as an approximately 100-fs duration, approximately nJ pulse with a spectrum centered at 1060 nm. The pulse travels to a multi-pass regenerative stretcher where it is temporally stretched to approximately 20 ns. From here, the beam is sent into a cylindrical telescope to expand the vertical dimension, creating a 2:1 aspect ratio, and then enters a single grating pair, composed of gratings identical to those in the compressor, that induces a 2× spatial chirp. The output of this is our chirped-beam pulse. Due to the unique gain effects present in CPJBA, the spatio-spectral distribution of the pulse must be appropriately sculpted^[ Reference Korman, Bahar, Arieli and Suchowski ^{70 ,} Reference Zhan ^{71 ]}. To further deal with spatial gain effects and amplifier inhomogeneities an adaptive optic allows for a spatial mask to be applied to the beam, similar to the NIF front-end^[ Reference Heebner, Borden, Miller, Hunter, Christensen, Scanlan, Hayman, Wegner, Hermann, Brunton, Tse, Awwal, Wong, Seppala, Franks, Marley, Williams, Budge, Henesian and Dinicola ^{72 ,} Reference Heebner, Acree, Alessi, Barnes, Bowers, Browning, Budge, Burns, Chang, Christensen, Crane, Dailey, Erbert, Fischer, Flegel, Golick, Halpin, Hamamoto, Hermann, Hernandez, Honig, Jarboe, Kalantar, Kanz, Knittel, Lusk, Molander, Pacheu, Paul, Pelz, Prantil, Rushford, Schenkel, Sigurdsson, Spinka, Taranowski, Wegner, Wilhelmsen, Nan Wong and Yang ^{73 ]}. A vast majority of the total system gain comes from a broadband OPCPA pre-amplifier, with a gain of 109, which also performs the bulk of the spectral sculpting on the highly stretched pulse by modulating the pump intensity in time^[ Reference Batysta, Antipenkov, Borger, Kissinger, Green, Kananavičius, Chériaux, Hidinger, Kolenda, Gaul, Rus and Ditmire ^{74 ,} Reference Lee, Kim, Yoo, Yoon, Yang, Lim, Nam, Sung and Lee ^{75 ]}. At this point the chirped-beam pulse has approximately 1 J of energy and is expanded to an aperture of 37 cm × 37 cm before entering the two separate large-aperture, NIF-like PA stages – a Nd:silicate stage followed by a Nd:phosphate stage^[ Reference Hays, Gaul, Martinez and Ditmire ^{51 ]}. The lens-based spatial filter currently used in the NIF amplifier is not suitable for short-pulse operation; instead, an entirely reflective spatial filter arrangement can be incorporated to minimize dispersion effects^[ Reference Chesnut, Bayramian, Erlandson, Galvin, Sistrunk, Spinka and Haefner ^{76 ]}. The now 20-ns, 25-kJ chirped-beam pulse travels through the six-grating compressor, split into 36 identical copies by a dispersion balanced beam splitter arrangement to 36 distributed final grating pairs, and emerges as 36, 18.5-cm by 37-cm aperture beamlets each with approximately 556 J of energy compressed down to a 100-fs FWHM FTL pulse duration for a total power of 0.2 EW. The beamlets are phased together using a multi-mirror focusing array; both a tiled parabolic focusing mirror, similar to those used by large-aperture telescopes^[ Reference Trumper, Hallibert, Arenberg, Kunieda, Guyon, Stahl and Kim ^{59 ]}, and a dipole focusing system^[ Reference Gonoskov, Bashinov, Gonoskov, Harvey, Ilderton, Kim, Marklund, Mourou and Sergeev ^{56 ]} have been discussed. The former, shown here, can focus to 10²⁵ W/cm², while the latter has been previously simulated with a 0.2-EW laser to achieve 10²⁶ W/cm^2[ Reference Gonoskov, Bashinov, Gonoskov, Harvey, Ilderton, Kim, Marklund, Mourou and Sergeev ^{56 ]}. This is, respectively, two and three orders of magnitude greater than the current world record. This focused intensity would push ultra-high-intensity lasers into the ultra-relativistic optics regime^[ Reference Mourou ^{77 ]}, and well within the quantum electrodynamics (QED) plasma regime^[ Reference Qu and Fisch ^{78 ]}.

For Nexawatt, we consider a pulse spectrum with an eighth-order super-Gaussian envelope to avoid clipping on the gratings or amplifier, centered at 1060 nm with 30.2-nm full width at half maximum (FWHM) – this will produce a 100-fs FWHM transform-limited sinc²-like temporal pulse. The spectral cutoff points, to handle the finite width of the grating, are defined as the spectral components with 1% of the peak spectral power. This results in a red-most wavelength of 1078 nm and a blue-most wavelength of 1042 nm. Clipping the spectrum here has minimal effect on the temporal pulse shape. The spectral pulse is shown in Figure 6. Spatially, the input beam to the six-grating compressor is a rectilinear eighth-order super-Gaussian with a width and height of 37 cm × 37 cm, at 1% peak fluence, as found on most large-aperture Nd:glass lasers^[ Reference Haynam, Wegner, Auerbach, Bowers, Dixit, Erbert, Heestand, Henesian, Hermann, Jancaitis, Manes, Marshall, Mehta, Menapace, Moses, Murray, Nostrand, Orth, Patterson, Sacks, Shaw, Spaeth, Sutton, Williams, Widmayer, White, Yang and Van Wonterghem ^{46 ]}. At the entrance of the compressor the beam has a spatial chirp of two that has been generated by an upstream grating pair. This spatial chirp distributes the spectral components across the transverse dimension, the x-position, of the beam as dictated by the grating equation, which follows a decidedly nonlinear distribution. This generates a larger spatial dispersion, ${\zeta \equiv \mathrm{d}{x}_0/\mathrm{d}\omega}$ , where ${x}_0$ is the center x-position of the frequency component $\omega$ , for the red end of the spectrum compared to the blue end of the spectrum^[ Reference Nelson, Chesnut, Reutershan, Effarah, Charbonnet and Barty ^{79 ]}. At the output of the six-grating compressor the spatial chirp has been undone and the beam emerges with a width and height of 18.5 cm × 37 cm, respectively.

Figure 6

Power spectrum of the original super-Gaussian pulse as well as the sculpted pulse that counteracts the asymmetry of the spatio-temporal pulse that arises from the large TOD of the ideal stretched pulse. The spectral phase of the stretched pulse and compressed pulse is shown as well.

Figure 7

Original super-Gaussian spectral pulse with ideal (a) spatio-spectral and (b) spatio-temporal input to the six-grating compressor. (c) Log intensity of the FTL temporal pulse of both the original and sculpted spectra. (d) Spatial distribution of the peak intensity across the transverse position of the beam for both the original and sculpted spectra.

Most of the modeling presented in this paper has been done by taking the desired sub-system output and propagating it backwards in time through the sub-system optical components, which gives the appropriate sub-system input. In our previous detailing of the six-grating compressor arrangement for Nexawatt^[ Reference Chesnut and Barty ^{63 ]}, the optimal spatio-spectral and spatio-temporal chirped-beam pulse distribution that can be compressed by this chirped-beam compressor arrangement was determined by back-propagating the desired final output pulse through the six-grating compressor using the ray trace software VirtualLab^{[ 80 ]}. An analysis plane after G1, the input to the six-grating compressor, collects the spatio-spectral intensity distribution, Figures 7(a) and 7(c), and spectral phase, Figure 6. A post-processing script in Python^[ Reference Van Rossum and Drake ^{81 ]} iterates through the spatial positions of the beam performing a Fourier transform on each spectral cross-section to produce the spatio-temporal intensity map seen in Figures 7(b) and 7(d). Webb et al. ^[ Reference Webb, Guardalben, Dorrer, Bucht and Bromage ^{82 ]} used a similar technique to simulate the effects of compressor grating misalignments on CPA systems. The temporal asymmetry seen in the spatio-temporal distribution is caused by the large amount of third-order dispersion (TOD) that is a consequence of any high-dispersion, grating-based stretcher–compressor system with this magnitude of temporal chirp. This spatial variation of the temporal intensity is not ideal for amplification as the highest intensity portion of the beam will accumulate the most B-integral and limit the amount of total energy that can be extracted. To homogenize the intensity distribution, and by extending the B-integral contribution, the spectrum can be red-shifted, as shown in Figures 6 and 7(c). This distributes more energy content to the earlier time positions in the stretched spatio-temporal pulse that travels through the amplifier, resulting in a flatter peak intensity distribution, Figure 7(d), while maintaining the same FTL pulse duration after compression.

4 Multi-pass regenerative stretcher

To safely extract the full stored approximately 26 kJ of energy from a single NIF PA requires a stretched pulse with duration greater than 20 ns^[ Reference Haynam, Wegner, Auerbach, Bowers, Dixit, Erbert, Heestand, Henesian, Hermann, Jancaitis, Manes, Marshall, Mehta, Menapace, Moses, Murray, Nostrand, Orth, Patterson, Sacks, Shaw, Spaeth, Sutton, Williams, Widmayer, White, Yang and Van Wonterghem ^{46 ]}. In practice, this stretch factor is difficult to achieve on few-pass stretchers as a nanosecond difference in group delay requires nanosecond size optics, which are meter-scale. Stretcher optics have stringent quality requirements, such as radius of curvature, surface flatness, roughness and so forth, to avoid wavefront aberrations propagating through the amplifier chain and maintain a high level of temporal intensity contrast. These two factors combined present a large engineering and financial challenge. Instead, by inducing only a small amount of GDD per pass and performing a high number of passes until the desired GDD is acquired, one can use reasonably sized optics. However, losses from the gratings, as well as other optics, will compound on each pass. Having sub-nJ pulses after stretching places considerable burden on the downstream OPCPA amplifier. By placing the stretcher inside the cavity of a regenerative amplifier one can create a high-pass stretcher that maintains, or amplifies, the pulse energy.

The major requirements of the regenerative stretcher for the Nexawatt system are to produce a stretched pulse of at least 20 ns, have a dispersion profile that is the conjugate of the compressor and total system material dispersion and minimize the creation of pre- and post-pulses that can propagate through the system, degrading the final temporal contrast. To date, two intracavity stretcher designs have been published. In 2017, Liebetrau et al. ^[ Reference Liebetrau, Hornung, Keppler, Hellwing, Kessler, Schorcht, Hein and Kaluza ^{83 ]} published an intracavity Offner-type stretcher producing a 3.9-ns, 100-μJ stretched pulse. However, the line focus produced on a secondary telescope mirror of the stretcher, inherent to any Offner-type stretcher, limited the pulse energy to avoid optical damage and led to degraded temporal intensity contrast in the ps-pedestal. At the convex mirror the beam is spatially chirped and focused to a small size, which imparts a spectral phase noise on the pulse due to mirror imperfections and manifests as a ps-scale slow-rising edge on the pulse^[ Reference Lu, Zhang, Li and Leng ^{84 ,} Reference Roeder, Zobus, Brabetz and Bagnoud ^{85 ]}. In 2019, Su et al. ^[ Reference Su, Peng, Li, Lu, Chen, Wang, Lv, Shao and Leng ^{86 ]} presented an intracavity Martinez-type stretcher demonstrating 10-ns, 5-mJ stretched pulses. This design utilized a simple hemispherical cavity that is susceptible to pulse overlap in the gain media. Pulse overlap creates a spectral interference leading to a modulation of the pulse phase and intensity generating a pre-pulse after compression^[ Reference Didenko, Konyashchenko, Lutsenko and Tenyakov ^{87 ,} Reference Kiriyama, Miyasaka, Sagisaka, Ogura, Nishiuchi, Pirozhkov, Fukuda, Kando and Kondo ^{88 ]}. The regenerative stretcher presented here, shown in Figure 8, uses a Martinez stretcher inside an optical cavity that places the gain media in a unidirectional, single-pass ring to better isolate it from pulse overlap and reduce the mode size in the crystal for more efficient pumping.

Figure 8

Schematic of the regenerative stretcher. The polarization state of the beam as it transverses the ring is denoted by the vector symbols.

Figure 9

Beam caustic in the tangential plane of the cavity mode supported by the regenerative stretcher using the physical parameters discussed in this section.

The pulse is coupled into, and out of, the regenerative stretcher by a thin-film polarizer (TFP) and a Pockels cell (PC) where it then travels through a Martinez stretcher. After double passing the stretcher, the pulse polarization is rotated from p-polarization to s-polarization by a Faraday rotator (FR) and a half-wave plate (HWP) to be reflected by a second TFP. Once reflected, the pulse is rotated back to p-polarization by an HWP so it can pass lossless through a Brewster cut Ti:sapphire crystal (Xtal) and back through the TFP. In this unidirectional single-pass ring, a one-to-one Keplerian telescope, formed by two 500-mm focal length concave mirrors (CMs) at 4-degree AOI for astigmatism compensation in the 12-mm long Brewster cut crystal, focuses the pulse for amplification. The Martinez stretcher must have a length greater than 3 m, for a double-pass length of 6 m, to fully contain the 20-ns stretched pulse on one side of the PC. In this paper we have used 500-mm achromat lenses as the focusing elements in the Martinez stretcher for simplicity of the cavity design and dispersion analysis; however, in practice the stretcher should be built with concave, circular mirrors to avoid the aberrations that come with the use of lenses^[ Reference Lemoff and Barty ^{89 ]}. Starting from the flat high-reflectivity (HR) mirror in the spectrally dispersed arm of the stretcher, a full round-trip in the cavity, shown in Figure 8, will double-pass the stretcher while passing through the gain element only once.

This regenerative stretcher cavity is essentially a four-mirror x-fold cavity where the two arms have been combined into one and only a single pass of the gain medium per round-trip. The total round-trip ABCD ray transfer matrix of the regenerative stretcher determines the stability limits of the cavity. We define the distance from the end mirror (HR) to the second grating (G2) as ${d}_1$ , the distance from the first grating (G1) to either curved mirror (CM1/2) as ${d}_2$ and the length of the Martinez stretcher, $2f-{s}_1-{s}_2$ , as ${L}_\mathrm{str}$ . Starting at the flat end mirror (HR), and breaking the cavity into the stretcher arm and the crystal ring, the total round-trip ABCD matrix is as follows:

(3) $$\begin{align}{\mathbf{M}}_\mathrm{Total}&={\mathbf{M}}_\mathrm{arm}{\mathbf{M}}_\mathrm{xtal}{\mathbf{M}}_\mathrm{arm}, \end{align}$$

(4) $$\begin{align}{\mathbf{M}}_\mathrm{arm}&=\left[\begin{array}{cc}-1& {L}_\mathrm{str}-{d}_1-{d}_2\\ {}0& -1\end{array}\right],\end{align}$$

(5) $$\begin{align}{\mathbf{M}}_\mathrm{xtal}&=\left[\begin{array}{cc}1-\frac{\varLambda }{\eta }& \varLambda \\ {}\frac{\varLambda }{\eta^2}-\frac{2}{\eta }& 1-\frac{\varLambda }{\eta}\end{array}\right].\end{align}$$

Here, both $\varLambda$ and $\eta$ have a different form in the tangential and sagittal planes. Namely,

(6) $$\begin{align}{\varLambda}_{\mathrm{s,t}}&=2{d}_3+\frac{l_\mathrm{xtal}}{n_\mathrm{xtal}},\ 2{d}_3+\frac{l_\mathrm{xtal}}{n_\mathrm{xtal}^3},\end{align}$$

(7) $$\begin{align}{\eta}_{\mathrm{s,t}}&=\frac{R}{2\cos \theta },\ \frac{R\cos \theta }{2},\end{align}$$

where ${l}_\mathrm{xtal}$ is the length of the crystal, ${n}_\mathrm{xtal}$ is the crystal index of refraction, ${d}_3$ is the distance from the curved mirror to the crystal face, $R$ is the curved mirror’s radius of curvature and $\theta$ is the AOI on the curved mirror. Like the four-mirror oscillator, the stability of the cavity and collimation of the cavity mode in the stretcher arm can be obtained by tuning the separation of the two curved mirrors. Defining ${\varLambda =2\eta +\delta}$ , the cavity stability can be defined in terms of a detuning parameter, $\delta$ , from a perfect telescope:

(8) $$\begin{align}0\le \delta \left(\frac{1}{\eta }-\frac{L_\mathrm{str}-{d}_1-{d}_2}{\eta^2}\right)\le 2.\end{align}$$

The cavity is stable when the detuning parameter is zero, and for many small values of $\delta$ as long as $\left({L}_\mathrm{str}-{d}_1-{d}_2\right)/\eta \le 1$ . This is better viewed by recasting the cavity stability in terms of the distances ${d}_1$ and ${d}_2$ allowed for some given detuning parameter and stretcher length:

(9) $$\begin{align}{L}_\mathrm{str}-\eta \le {d}_1+{d}_2\le \left({L}_\mathrm{str}-\eta \right)+\frac{2{\eta}^2}{\delta }.\end{align}$$

When $\delta$ is small, this cavity design supports a wide range of mirror spacings ${d}_1$ and ${d}_2$ , making it relatively insensitive to changes in these mirror spacings. In the design presented here, ${d}_1$ is 764.5 mm, ${s}_1$ and ${s}_2$ equal 435.5 mm, ${d}_2$ is 1064.5 mm and the detuning parameter $\delta$ is approximately 14.4 mm in the sagittal plane and approximately 14.7 mm in the tangential plane. This equates to a cavity stability parameter of approximately 0.126 in the sagittal plane and approximately 0.130 in the tangential plane. The cavity caustic for the particular spacing and geometry described here is shown in Figure 9.

Here, the stretcher is designed to generate approximately 1 ns of stretch on the temporal pulse per round-trip pass. The transmissive optics in a NIF-like beamline, along with the intracavity optical elements of the regenerative stretcher, impart additional material dispersion that cannot be compensated by an identical stretcher–compressor pair. This can largely be accounted for by modifying the groove density and AOI of the stretcher gratings^[ Reference Lemoff and Barty ^{89 ,} Reference Kane and Squier ^{90 ]}. Table 1 lists the GDD and TOD contributions of each element in the regenerative stretcher, the six-grating CPJBA compressor and the reported material dispersion of a NIF beamline^[ Reference Williams, Crane, Alessi, Boley, Bowers, Conder, Di Nicola, Di Nicola, Haefner, Halpin, Hamamoto, Heebner, Hermann, Herriot, Homoelle, Kalantar, Lanier, LaFortune, Lawson, Lowe-Webb, Morrissey, Nguyen, Orth, Pelz, Prantil, Rushford, Sacks, Salmon, Seppala, Shaw, Sigurdsson, Wegner, Widmayer, Yang and Zobrist ^{91 ]}. Furthermore, the 2× spatial chirp required for CPJBA is created by a parallel grating pair with the same design as the final compressor gratings, 1780-line/mm groove density and 76.5-degree AOI, after the regenerative stretcher. The additional negative dispersion created by the grating pair can be compensated by over stretching the pulse. A parameter scan was performed on the regenerative stretcher grating groove density and AOI to determine the optimal configuration that balances all GDD in the system while minimizing the TOD contribution. This first-pass optimization suggests the use of 1760-line/mm groove density gratings at a 71.85-degree AOI, which allows for full GDD compensation of the system with a residual TOD of –4.94 × 10⁵ fs³. This residual TOD would broaden the final 100-fs TFL output pulse to 102.6 fs. A breakdown of the GDD and TOD contributions of the various components of the Nexawatt laser chain is shown in Table 1. Through further optimization of the regenerative stretcher, such as modifications to the spherical mirrors in the stretcher^[ Reference Lemoff and Barty ^{89 ]}, one can fully compensate the residual TOD; however, that analysis is beyond the scope of the paper as it requires accurate knowledge of the full system design. Using 500-mm focal length achromat lenses, the 2f−2s length in this stretcher design is 129.8 mm, and with the above grating configuration generates the appropriate GDD to stretch the pulse to 20 ns after 20 round-trip passes.

Table 1

Tabulation of the GDD and TOD contribution of the regenerative stretcher intracavity components and the rest of the Nexawatt laser chain for the full system dispersion^a.

^aDKDP, deuterated potassium dihydrogen phosphate; TGG, terbium gallium garnet; N-BAK4, Schott light barium crown glass; N-SF10, Schott dense flint glass.

5 Chirped pulse juxtaposed with beam amplification energetics

5.1 Energetics modeling

CPJBA is unique in its amplification of a highly temporally stretched, spatially chirped beam. An amplification model capable of handling a custom spatio-temporal field was developed to demonstrate these effects. The amplification model is based on a numerical implementation of the Frantz–Nodvik solution, which describes the gain dynamics of a square-shaped temporal pulse in an amplifier^[ Reference Frantz and Nodvik ^{92 ]}. This solution is extended to temporal pulses of arbitrary shape by modeling them as a collection of discrete square pulses of width $\Delta t$ and varying amplitude^[ Reference Jeong, Cho, Hwang, Lee and Yu ^{93 ]}. The square pulses are treated consecutively by the Frantz–Nodvik solution, Equation (11), with each modifying the remaining population inversion and, thus, the gain that the subsequent experiences, Equation (12). The high temporal stretch factor means each unit of time in the pulse corresponds to a different wavelength with a different emission cross-section in Nd:APG-1. Thus, each of our square pulses in time will have different small-signal gain and gain saturation. The group delay of each wavelength is calculated from the spectral phase of the pulse that is compressed by the six-grating compressor. This correlates each of the discrete square temporal pulses with the correct spectral wavelength. Due to the spatial chirp the gain effects need to be considered transversely across the beam as well. This is done by breaking the beam and amplifier medium into a transverse grid, with spacing $\Delta x$ , and recording the beam energy and population inversion along this coordinate.

The amplification model is initialized by defining the transverse spatial distribution of the stored energy in the amplifier, which sets the starting population inversion at each spatial location ${x}_i$ . The script iterates over each of these spatial points, taking the temporal cross-section at that location and breaking the temporal pulse into a sequence of square pulses, as shown in Figure 10, where they are consecutively amplified according to the Frantz–Nodvik solution. With this, our coupled gain and population inversion equations are as follows:

(10) $$\begin{align}{E}_\mathrm{out}\left({x}_i,{t}_n\right)={E}_\mathrm{in}\left({x}_i,{t}_n\right)G\left({x}_i,{t}_n\right),\end{align}$$

(11) $$\begin{align}{E}_\mathrm{out}&={E}_\mathrm{sat}\ln \Big\{1+\left[\exp \left(\frac{E_\mathrm{in}\left({x}_i,{t}_n\right)}{E_\mathrm{sat}\left({t}_n\right)}\right)-1\right]\nonumber\\&\qquad\qquad \times\exp \left[N\left({x}_i,{t}_n\right)\sigma \left({t}_n\right)L\right]\Big\},\end{align}$$

(12) $$\begin{align}&N\left({x}_i,{t}_{n+1}\right)=N\left({x}_i,{t}_n\right)\nonumber\\ & \quad -\left[{E}_\mathrm{out}\left({x}_i,{t}_n\right)-{E}_\mathrm{in}\left({x}_i,{t}_n\right)\right]\frac{1}{L}.\end{align}$$

Figure 10

(a) Input spatio-temporal intensity distribution to the amplification code that iterates over the spatial distribution with discretized segments of width $\Delta x$ , which produce (b) temporal cross-sections that are modeled as a collection of square temporal pulses, of width $\Delta t$ , to be treated by the Frantz–Nodvik solution.

Here, ${E}_{\mathrm{out}}$ ( ${x}_i$ , ${t}_n$ ) and ${E}_{\mathrm{in}}$ ( ${x}_i$ , ${t}_n$ ) are the beam output and input energy, respectively, ${E}_{\mathrm{sat}}$ ( ${t}_n$ ) is the saturation fluence of the pulse, N( ${x}_i$ , ${t}_n$ ) is the population inversion, $\sigma$ ( ${t}_n$ ) is the emission cross-section and L is the length of the amplifier. In our simplified model we ignore ASE, transient pumping effects, thermal gain effects and phase distortion from the atomic phase shift in the amplifier. Our spatio-temporal simulation grid is broken into 200 spatial points, of $\Delta x$ width of approximately 1.89 mm, and 500 temporal points of $\Delta t$ width of approximately 0.11 ns. To calculate the B-integral, defined in Equation (13), the total length, L, of the amplifier is divided into sections $\Delta z$ of length 10 mm. At each section $\Delta z$ of the amplifier the local peak intensity is used to generate that segments contribution to the B-integral:

(13) $$\begin{align}B=\frac{2\pi }{\lambda }{n}_2{\int}_0^{L}I(z)\kern0.1em \mathrm{d}z=\frac{2\pi }{\lambda }{n}_2\sum \limits_{z=0}^{z=n}{I}_{\mathrm{peak},z}\Delta z.\end{align}$$

As described in Section 2, the output pulse spectrum is an eighth-order super-Gaussian envelope, to avoid clipping on the gratings or amplifier, centered at 1060 nm with 30.2-nm FWHM – this will produce a 100-fs FWHM transform-limited sinc² temporal pulse. Spatially, each beamlet emerging from the six-grating compressor is a rectilinear, eighth-order super-Gaussian with a width of 18.5 cm and height of 37 cm. A 2× spatial chirp, induced prior to the six-grating compressor and amplifier, produces a 37-cm × 37-cm beam, which is comparable to the aperture size of most high-energy Nd:glass lasers^[ Reference Neauport, Airiau, Beck, Belon, Bordenave, Bouillet, Chanal, Chappuis, Coic, Courchinoux, Denis, Gaudfrin, Gaudfrin, Gendeau, Heymans, Julien, Lacombe, Lamy, Lebeaux, Luttmann, Modelin, Perrin, Ribeyre, Rouyer, Tournemenne, Valla and Vermersch ^{47 ,} Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}. The input pulse energy is set to 40 J to match the previous energetics study on high-energy, broadband Nd:mixed-glass amplifiers^[ Reference Hays, Gaul, Martinez and Ditmire ^{51 ]}. The amplifier system is modeled after the architecture of a single NIF beamline with a four-passed MA and a double-passed PA – the PA is passed through once before and once after the four passes on the MA^[ Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}. All slabs are composed of Nd:APG-1, each 4-cm thick with an on-beam aperture of 37 cm × 37 cm and a Nd doping concentration of 4.22 × 10²⁰ ions/cm^3 [ Reference Suratwala, Campbell, Miller, Thorsness, Riley, Ehrmann and Steele ^{94 ]}. Pulse amplification depends only on the total stored energy and is agnostic to the total path length in the amplifier insofar as energy is concerned. The total number of slabs will modify the ASE and B-integral^[ Reference Haney, Williams, Sacks, Orth, Auerbach, Lawson, Henesian, Jancaitis, Renard and Trenholme ^{95 ,} Reference Caird, Agrawal, Bayramian, Beach, Britten, Chen, Cross, Ebbers, Erlandson, Feit, Freitas, Ghosh, Haefner, Homoelle, Ladran, Latkowski, Molander, Murray, Rubenchik, Schaffers, Siders, Stappaerts, Sutton, Telford, Trenholme and Barty ^{96 ]}, while not affecting the amplified pulse structure. We initially consider the ‘11-7’ configuration – eleven MA slabs and seven PA slabs^[ Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}. In the amplifier, the pulse will travel through a spatial filter after the first passes in the PA, after the first and second passes in the MA, again after the third and fourth passes in the MA, then once again after the second PA pass^[ Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}.

5.2 CPJBA amplification effects

To illustrate the CPJBA amplification effects, the spatio-temporal distribution shown in Figure 7(d), with a total energy of 40-J, is sent into the amplifier. Using a flat initial spatial gain distribution in the amplifiers (i.e., the stored energy in the amplifier slabs is spatially uniform across the transverse dimension of the slabs) with an initial stored energy of 22.7 kJ in the MA and 14.445 kJ in the PA, will amplify the chirped-beam pulse to 25 kJ with the resulting spatio-temporal distribution as shown in Figure 11(a). This corresponds to a total stored energy of 37.145 kJ in the amplifiers and an efficiency of 67.3%. The output exhibits significant pulse distortions from the desired amplified pulse due to a combination of gain narrowing and gain saturation. Both effects are ubiquitous to broadband, high-gain amplification; however, they have a unique presentation in CPJBA. Gain narrowing, a process where the spectral components at the peak of the emission cross-section curve experience higher gain than the spectral wings^[ Reference Hotz ^{97 ]}, results in a lack of pulse content at the temporal edges of the amplified pulse shown in Figure 11(a). This causes the FWHM pulse duration at the middle of the beam to be reduced from 20.6 to 9.51 ns, as shown in Figure 11(c). Temporal pulse distortion due to gain saturation is a well-known phenomenon in CPA laser amplifiers^[ Reference Cabezas, McAllister and Ng ^{98 ,} Reference Schimpf, Seise, Limpert and Tünnermann ^{99 ]}. When operating near the saturation fluence of the gain media, the leading edge of the temporal pulse will deplete the population inversion of the amplifier before the trailing edge arrives, leading to higher gain and distortion of the temporal pulse shape.

Figure 11

(a) Spatio-temporal intensity distribution in units of W/cm² of the amplified 25-kJ output pulse. (b) Cross-section A at x = 110 mm with an FWHM duration of 2.54 ns. (c) Cross-section B at x = 0 mm with an FWHM duration of 9.51 ns. (d) Cross-section C at x = –95 mm with an FWHM of 5.60 ns. The dashed lines indicate the temporal evolution of the stored energy of both the main and power amplifier slabs on each pass.

In CPJBA, the spatial chirp induces a spatial dependence on the temporal position of the leading edge. Now, the spectral components at the emission cross-section peak are exposed to the full stored energy in the amplifier, and hence gain, before the spectral components with lower emission cross-section can deplete it. Along with the spatial energy distribution of the pulse, this leads to a varying effective gain across the transverse profile of the beam producing the asymmetric amplified pulse energy fluence distribution, seen in Figure 12(b), which significantly varies from the goal-amplified pulse energy fluence. Since the spatial edges of the beam have a reduced FWHM pulse duration, an intensity hot spot develops on the leading-edge side of the beam corresponding to the temporal position of the 1053-nm component of the pulse spectrum (i.e., the emission cross-section and gain maximum). This results in a large B-integral accumulation, shown in Figure 12(d), at the spatial position of the intensity hot spot with a peak of 17.75.

Figure 12

Spatial distribution of (a) initial and final stored energy fluence in the MA and PA, (b) the amplified pulse fluence comparing the base case input pulse output to the goal-amplified pulse, (c) peak intensity of the amplified output pulse and (d) the total accumulated B-integral during amplification.

Figure 13

The first case of a flat distribution of remaining stored energy in the MA and PA. (a) Log intensity of the 40-J input pulse spatio-temporal profile sent into the NIF-like final amplifier with an (b) initial stored energy fluence spatial distribution in the MA and PA. This results in (c) the amplified 25-kJ output pulse spatio-temporal profile and (d) a final stored energy fluence spatial distribution in the MA and PA. (e) Spatial distribution of the total B-integral accumulated during amplification for this configuration.

The temporal and spatial pulse distortion effects present in CPJBA due to amplification can be compensated by appropriately shaping both the input pulse and transverse gain distribution in the amplifier. This gain saturation effect is compensated by appropriately sculpting the spectrum of the input pulse to the amplifier, skewing the input power spectrum to the shorter wavelength components^[ Reference Schimpf, Seise, Limpert and Tünnermann ^{99 ]}. In the Nexawatt system, spectral sculpting can be accomplished in the broadband OPCPA stage. The temporal distribution of the spectrum in this highly stretched 20-ns pulse enables control of the gain of the different spectral components by modifying the temporal shape of the pump pulse^[ Reference Batysta, Antipenkov, Borger, Kissinger, Green, Kananavičius, Chériaux, Hidinger, Kolenda, Gaul, Rus and Ditmire ^{74 ,} Reference Lee, Kim, Yoo, Yoon, Yang, Lim, Nam, Sung and Lee ^{75 ]}. This is readily achieved with current multi-joule, ns-duration narrowband lasers and low-capacitance (i.e., fast switching) electro-optic cells. While this technique can perform the bulk of the spectral shaping, with a single PC supporting an extinction ratio of greater than or equal to 5000:1, this will only allow for a single spectral sculpting shape across the entire spatial extent of the beam. However, there are a number of 2D pulse shaping methods to fine tune the spatio-spectral distribution of the input pulse to the amplifier (i.e., a unique spectral sculpt profile at different transverse spatial positions on the beam)^[ Reference Korman, Bahar, Arieli and Suchowski ^{70 ,} Reference Zhan ^{71 ]}. These 2D pulse shapers take the traditional 4f pulse shaper, essentially a Martinez stretcher with s ${}_1$ = s ${}_2$ = f and an amplitude modulator at the Fourier plane between two lenses, and replace the one-dimensional (1D) amplitude modulator with a 2D device such as a diffractive optical element or digital micromirror device. This enables the spectral content of the pulse to be modulated along one of the transverse spatial coordinates of the beam^[ Reference Zhan ^{71 ]}.

The spatial pulse distortions during amplification can be addressed by two different methods – spatially shaping the beam prior to amplification and spatially varying the gain within the amplifier. The pre-amplifier modules (PAMs) at the NIF incorporate a programmable spatial shaper (PSS) that is composed of a system of specialty spatial light modulators, which allows for the blocking of portions of the low-fluence beam that correspond to the location of damage sites that are present on the downstream optics^[ Reference Heebner, Borden, Miller, Hunter, Christensen, Scanlan, Hayman, Wegner, Hermann, Brunton, Tse, Awwal, Wong, Seppala, Franks, Marley, Williams, Budge, Henesian and Dinicola ^{72 ,} Reference Heebner, Acree, Alessi, Barnes, Bowers, Browning, Budge, Burns, Chang, Christensen, Crane, Dailey, Erbert, Fischer, Flegel, Golick, Halpin, Hamamoto, Hermann, Hernandez, Honig, Jarboe, Kalantar, Kanz, Knittel, Lusk, Molander, Pacheu, Paul, Pelz, Prantil, Rushford, Schenkel, Sigurdsson, Spinka, Taranowski, Wegner, Wilhelmsen, Nan Wong and Yang ^{73 ]}. This system has demonstrated an optical density (OD) attenuation factor of OD 2 with mm-scale spatial resolution and extension to OD 5 is reasonable. In addition to the PSS, the NIF also incorporates a static spatial mask prior to the MA to account for the nonuniform small-signal spatial gain profile^[ Reference Heebner, Borden, Miller, Hunter, Christensen, Scanlan, Hayman, Wegner, Hermann, Brunton, Tse, Awwal, Wong, Seppala, Franks, Marley, Williams, Budge, Henesian and Dinicola ^{72 ,} Reference Heebner, Acree, Alessi, Barnes, Bowers, Browning, Budge, Burns, Chang, Christensen, Crane, Dailey, Erbert, Fischer, Flegel, Golick, Halpin, Hamamoto, Hermann, Hernandez, Honig, Jarboe, Kalantar, Kanz, Knittel, Lusk, Molander, Pacheu, Paul, Pelz, Prantil, Rushford, Schenkel, Sigurdsson, Spinka, Taranowski, Wegner, Wilhelmsen, Nan Wong and Yang ^{73 ]}. The easiest way to modify the spatial gain profile in the amplifier slabs is to shape the spatial profile of the pump fluence. The flash lamp pumps on the MA slabs of the NIF utilize a carefully designed, multi-curved reflector to distribute the pump energy more evenly, producing a more spatially uniform small-signal gain^[ Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}. For CPJBA, the desired spatial gain profile can be made nonuniform to compensate for the spatial pulse distortions. Moving to a diode pump source, as is common with current high-intensity Nd:glass lasers^[ Reference Reagan, Albrecht, Alessi, Ammons, Banerjee, Barillas, Batysta, Buckley, Chemali, Clark, Davila, Deri, Eseltine, Fishler, Fulkerson, Galbraith, Galvin, Gonzales, Gopalan, Herriot, Hubka, Jimenez, Kiani, Koh, Kupfer, Liao, Lusk, Nguyen, Patel, Peer, Peterson, Plummer, Schaffers, Sistrunk, Spinka, Stolz, Tamer, Tang, Telford, Terzi, Utley, Velas, Vella and Wong ^{49 ,} Reference Caird, Agrawal, Bayramian, Beach, Britten, Chen, Cross, Ebbers, Erlandson, Feit, Freitas, Ghosh, Haefner, Homoelle, Ladran, Latkowski, Molander, Murray, Rubenchik, Schaffers, Siders, Stappaerts, Sutton, Telford, Trenholme and Barty ^{96 ]}, will allow for greater control over the spatial distribution of the gain profile.

5.3 Nexawatt amplification

Conveniently, the Frantz–Nodvik solution is reversible^[ Reference Spaeth, Manes, Kalantar, Miller, Heebner, Bliss, Spec, Parham, Whitman, Wegner, Baisden, Menapace, Bowers, Cohen, Suratwala, Di Nicola, Newton, Adams, Trenholme, Finucane, Bonanno, Rardin, Arnold, Dixit, Erbert, Erlandson, Fair, Feigenbaum, Gourdin, Hawley, Honig, House, Jancaitis, LaFortune, Larson, Le Galloudec, Lindl, MacGowan, Marshall, McCandless, McCracken, Montesanti, Moses, Nostrand, Pryatel, Roberts, Rodriguez, Rowe, Sacks, Salmon, Shaw, Sommer, Stolz, Tietbohl, Widmayer and Zacharias ^{67 ]}. This allows one to specify the remaining stored energy in the amplifier and the desired amplified output pulse to obtain the ideal input pulse and initial stored energy. The inverse Frantz–Nodvik solution takes the following form:

(14) $$\begin{align}{E}_\mathrm{in}\left({x}_i,{t}_n\right)&={E}_\mathrm{sat}\ln \Big\{1+\left[\exp \left(\frac{E_\mathrm{out}\left({x}_i,{t}_n\right)}{E_\mathrm{sat}\left({t}_n\right)}\right)-1\right]\nonumber\\&\qquad\qquad\times\frac{1}{\exp \left[N\left({x}_i,{t}_n\right)\sigma \left({t}_n\right)L\right]}\Big\},\end{align}$$

(15) $$\begin{align}&\quad N\left({x}_i,{t}_{n-1}\right)=N\left({x}_i,{t}_n\right)+\left[{E}_\mathrm{in}\left({x}_i,{t}_n\right)+{E}_\mathrm{out}\left({x}_i,{t}_n\right)\right]\frac{1}{L}.\end{align}$$

The desired output spatio-temporal intensity distribution, scaled to 25 kJ in Figure 13(c), is a fixed input, while the spatial distribution of the remaining stored energy in each amplifier section, post-amplification, is a free variable. This desired, amplified spatio-temporal pulse distribution is then back-propagated through the amplifier using the inverse Frantz–Nodvik solution. Each supplied final energy distribution results in a unique, ideal spatio-temporal pulse input and initial stored energy distribution. Optimization is contingent on real-world design constraints, which are currently not material, and this section seeks, instead, to demonstrate the amplification dynamics.

We first consider the case of a spatially flat final stored energy distribution, Figure 13(d), with remaining energy split between the MA and PA at a ratio that produces approximately the same initial energy per slab in both the MA and PA for the ‘11-7’ amplifier configuration. The total remaining energy determines the input pulse energy; a lower amount of remaining stored energy in the amplifier (i.e., more efficient energy extraction) requires a higher input pulse energy. Here it is set to 10.4 kJ to give an input pulse energy of 40 J, which is commensurate with previous studies on potential exawatt-class Nd:glass lasers^[ Reference Hays, Gaul, Martinez and Ditmire ^{51 ]}. Using this final stored energy distribution of the amplifier and back-propagating the desired amplified output pulse using the inverse Frantz–Nodvik solution produces the input pulse spatio-temporal distribution, Figure 13(a), as well as the initial stored energy distribution in the amplifiers, shown in Figure 13(b). This input pulse, in combination with the initial stored energy distribution, will result in the amplified spatio-temporal output pulse distribution, shown in Figure 13(c). The initial stored energy distribution has a total energy of approximately 36.76 kJ for an efficiency of 68.0%, and is free of any high-frequency spatial modulations, allowing for gain shaping with a diode pump source. In addition to producing a nearly ideal amplified output pulse, this arrangement has a peak B-integral value of approximately 3.5 with a relatively flat spatial distribution – well within the acceptable limits of large-aperture Nd:glass lasers. While the spatio-temporal distribution of this input pulse is quite different from pulse structures normally used during amplification, Figures 14(a)–14(f) show how the pulse evolves during the various passes through the MA and PA, culminating in the desired amplified output pulse spatio-temporal distribution.

Figure 14

Evolution of the spatio-temporal pulse distribution during amplification given the input pulse seen in Figure 13(a) and initial stored energy distribution in Figure 13(b).

One can control the input pulse spatio-temporal profile by modifying the remaining stored energy spatial distribution in the amplifier. Increasing the amount of remaining stored energy at a particular transverse position in the amplifier will decrease the necessary energy of the input pulse at the same location, lowering the pulse intensity there. This can allow for an input spatio-temporal pulse profile with lessened sculpting requirements. To demonstrate, the inverse of the goal output pulse’s spatial energy distribution, seen in Figure 12(b), is used as the remaining stored energy spatial distribution, shown in Figure 15(d). For an input pulse of 40 J and initial stored energy split evenly for the ‘11-7’ configuration, a total stored energy of approximately 34.46 kJ is required, equating to a 72.5% amplification efficiency – 4.5% greater than the flat remaining stored energy case above. Increasing the remaining energy on the spatial edges of the amplifier and reducing the energy on the center lowers the sculpting requirements on the pulse, as seen in the input pulse spatio-temporal intensity distribution, Figure 15(a). While this arrangement has greater efficiency and reduced sculpting requirements, it does have a larger peak B-integral value of approximately 5.

Figure 15

The second case of a modified distribution of remaining stored energy in the MA and PA with reduced remaining energy on the center. (a) Log intensity of the 40-J input pulse spatio-temporal profile sent into the NIF-like final amplifier with an (b) initial stored energy fluence spatial distribution in the MA and PA. This results in (c) the amplified 25-kJ output pulse spatio-temporal profile and (d) a final stored energy fluence spatial distribution in the MA and PA. (e) Spatial distribution of the total B-integral accumulated during amplification for this configuration.

6 Multi-beam focusing system

Prior to the final compressor grating pair the pulse must be split into multiple identical copies to lower the fluence of each beamlet below the damage threshold of the gratings. This can be accomplished with a cascading beam splitter arrangement, shown in Figure 16, where each beamlet is transmitted through a beam splitter only once to ensure all copies experience the same dispersion response. Prior to splitting the beam will be 37 cm × 37 cm with approximately 21.6 kJ of energy, after diffraction losses, for a fluence of 16.5 J/cm², and partially temporally compressed to a pulse duration of 3.3 ns.

Figure 16

Unit cell of the dispersion balanced beam splitting arrangement that splits the amplified chirped-beam pulse into 36 copies prior to final compression by the last grating pair in the six-grating compressor.

Leveraging the past few decades of experience developing high-quality MLD coatings, substantial research effort is being made today to push the size and laser-induced damage threshold (LIDT) of both electron beam evaporation (EBE) and ion beam sputtered (IBS) MLD coatings for high-energy inertial confinement fusion lasers and high-intensity petawatt lasers^[ Reference Oliver, Rigatti, Noll, Spaulding, Hettrick, Gruschow, Mitchell, Sadowski, Smith and Charles ^{100 –} Reference Laurence, Alessi, Feigenbaum, Negres, Qiu, Siders, Spinka and Stolz ^{102 ]}. Current industry leaders can supply large-aperture (i.e., $>$ 40 cm diameter) MLD coated beam splitters with high surface uniformity, substrate thickness tolerances of less than 100 μm and reflectivity variable from 0.2% to 99.5%^{[ 103 , 104 ]}. HR mirrors are capable of an LIDT of more than 80 J/cm² at 1064-nm, 10-ns pulses^{[ 103 ]}. However, coatings designed for partial reflectivity have a reduced LIDT compared to HR mirrors, which scales with reflectivity, with 50-50 beam splitters having an LIDT as low as 15 J/cm². For this reason, the first beam splitter arrangement should start with the highest reflectivity (i.e., 97.2% reflection to transmit 1/36 of the pulse energy) and decrease from there. While each beamlet will have the same number of transmissions they will have an uneven number of reflection events, making the wavefront quality of the beam splitters critical. Recently, large-scale anti-reflection (AR) metasurfaces have been written onto fused silica demonstrating an enhanced LIDT compared to traditional MLD AR coatings^[ Reference Ray, Yoo, Nguyen, Norton, Cross, Carr and Feigenbaum ^{105 ]}; this technique, applied to the backside of the beam splitter, would further extend the power handling capabilities of these optics. The exact design and optimization of this beam splitter arrangement are subject to further work. In particular, careful design is required to handle the minor reflectivity from the backside AR coatings causing back reflections that can interfere with the main pulse. This would lead to possible pre- and post-pulse generation as well as modulations to the near-field, and is a major challenge in high-intensity lasers with multiple transmissive optical components.

The ARC grating design has undergone extensive damage testing^[ Reference Britten ^{54 ,} Reference Alessi, Carr, Hackel, Negres, Stanion, Fair, Cross, Nissen, Luthi, Guss, Britten, Gourdin and Haefner ^{55 ]}. For longevity of the grating, actual operational fluence should not occur at the LIDT, but at a much lower fluence where damage is statistically unlikely. On the ARC design the operational fluence was set at the point where a 10^–4 fraction of the beam causes damage. Extrapolating the grating damage threshold trend, we estimate that the MLD gratings can handle approximately 1 J/cm² at 100 fs. With a final beamlet size of 18.5 cm × 37 cm each can have a maximum energy of approximately 685 J to stay below the grating damage threshold. With an estimated grating efficiency of approximately 97.5% the extracted approximately 25.1 kJ will be reduced to approximately 21.6 kJ after the sixth grating. Splitting the pulse into 36 beamlets, the fluence on the final grating, G6, will be approximately 600 J and below the operational fluence limit.

Phasing the 36 identical beamlets together is carried out by an appropriate focusing arrangement. In 2014, Gonoskov et al. ^[ Reference Gonoskov, Bashinov, Gonoskov, Harvey, Ilderton, Kim, Marklund, Mourou and Sergeev ^{56 ]} presented a technique called anomalous radiative trapping (ART) where multiple ultra-high-intensity beams are focused together to approximate an electric dipole. In this simulation they showed that a 200-PW laser split into multiple channels can reach a focused intensity greater than 10²⁶ W/cm². While this setup would provide the theoretical maximum focused field intensity, it has yet to be experimentally demonstrated. Here we examine a more traditional focusing arrangement, shown in Figure 17, where a large-aperture parabolic mirror is created by tiling together multiple, smaller individual mirror segments. This technique has already been put into practice by the large-aperture telescope community^[ Reference Trumper, Hallibert, Arenberg, Kunieda, Guyon, Stahl and Kim ^{59 ]}. The telescope tiled mirror segments have been produced at the meter scale with clear apertures of approximately 98%^[ Reference Martin, Allen, Burge, Davis, Davison, Johns, Kim, Kingsley, Law, Lutz, Strittmatter, Su, Tuell, West and Zhou ^{106 ]}. Each beamlet is focused by an individual mirror segment of modest f-number, that when tiled together produces a low f-number parabolic mirror. Phasing now becomes a three degree-of-freedom issue needing, in principle, approximately 100 nm of accuracy for alignment instead of the five degree-of-freedom problem with 10 nm of accuracy needed for tiling multiple gratings together^[ Reference Cong, Qi, Xu, Qiao, Mi, Li, Yu, Zhahng, Yu and Bayanheshig ^{36 –} Reference Cotel, Castaing, Pichon and Le Blanc ^{38 ]}.

Figure 17

(a) Near-field distribution of the 36 beamlets prior to focusing. (b) Rendering of the tiled parabolic focusing mirror for Nexawatt.

A custom beam propagation script was written in Python^[ Reference Van Rossum and Drake ^{81 ]} to evaluate the tiled parabolic mirror as a focusing system for the Nexawatt laser. The fields are defined before the focusing optic and propagated to the focus using Rayleigh–Sommerfeld propagation^[ Reference Voelz ^{107 ]}. The Bluestein method^[ Reference Hu, Wang, Wang, Ji, Zhang, Li, Zhu, Wu and Chu ^{108 ]} is used for calculating the numerical Fourier transforms, which allows for an arbitrarily sampled input and focal plane, relaxing the computational requirements for simulating very low f-number focusing systems. In this model the 36 mirror segments are spaced 5 mm apart, each with an aperture of 19 cm × 38.5 cm. The tiled parabolic mirror assembly is set to a focal length of 198.5 cm, giving an effective f-number of 0.95 in the horizontal dimension and 0.89 in the vertical dimension. The f-numbers of the individual segments are much more modest, with 10.6 in the horizontal dimension and 5.6 in the vertical dimension. This focusing system, with the input beam spatial profile shown in Figure 17(a), produces the far-field distribution shown in Figure 18(a). The focal spot has a 1/e² width of 3.41 μm in both the x-axis and y-axis, and a peak intensity exceeding 1 × 10²⁵ W/cm² – two orders of magnitude beyond the current record.

Figure 18

Beam intensity at the focus of the tiled on-axis parabolic mirror showing the (a) far-field intensity distribution, (b) the cross-section at the center in the X-direction and (c) the cross-section at the center in the Y-direction.

In laser–matter experiments, solid targets can begin generating a pre-plasma at intensities from 10¹⁰ to 10¹³ W/cm², and some research suggests pre-pulses as low as 10⁸–10⁹ W/cm² can have significant effects^[ Reference Wharton, Boley, Komashko, Rubenchik, Zweiback, Crane, Hays, Cowan and Ditmire ^{109 ]}. With a focused intensity of 10²⁵ W/cm² this calls for the temporal contrast of the pulse to be from 10^–12 to 10^–17 W/cm². Considerable research into improving the temporal contrast of ultra-high-intensity lasers has resulted in current PW laser systems operating with a picosecond pedestal contrast of 10¹⁰–10¹² W/cm^2 [ Reference Chalus, Derycke, Charbonneau, Pasternak, Ricaud, Fischer, Scutelnic, Gaul, Korn, Norbaev, Popa, Vasescu, Toma, Cojocaru and Dancus ^{110 –} Reference Kiriyama, Miyasaka, Kon, Nishiuchi, Sagisaka, Sasao, Pirozhkov, Fukuda, Ogura, Kondo, Nakanii, Mashiba, Dover, Chang, Kando, Bock, Ziegler, Püschel, Schlenvoigt, Zeil and Schramm ^{112 ]}. Incorporation of a plasma mirror has improved the contrast of the J-KAREN-P PW laser to an estimated value 10^15 [ Reference Kiriyama, Miyasaka, Kon, Nishiuchi, Sagisaka, Sasao, Pirozhkov, Fukuda, Ogura, Kondo, Nakanii, Mashiba, Dover, Chang, Kando, Bock, Ziegler, Püschel, Schlenvoigt, Zeil and Schramm ^{112 ]}, while the CoReLs 4-PW laser has reported a contrast of 10¹⁷ using a double plasma mirror^[ Reference Choi, Jeon, Lee, Kim, Kim, Kim, Lee, Yoon, Sung, Lee and Nam ^{113 ]}. Moving toward an exawatt-class laser will require careful consideration of all pre- and post-pulse sources, as well as an extension of existing, and new, temporal pulse contrast enhancement techniques.

In the tiled parabolic mirror array, each mirror segment will be positioned using three piezo-electric actuators on the rear allowing for adjustments to the tip, tilt and piston. The challenge of co-phasing the individual segments together to create the desired, ideal mirror shape is identical to that for large-aperture telescopes. To address this issue, multiple co-phasing techniques have been developed and employed^[ Reference Chanan, Troy and Sirko ^{114 –} Reference Cheetham, Tuthill, Sivaramakrishnan and Lloyd ^{116 ]}. In particular, a technique called Fizeau interferometric co-phasing of segmented mirrors (FICSM) has numerically shown the potential to co-phase mirror segments with initial piston errors of 300 μm and tip–tilt error of 0.5 arcseconds to final state with a root mean square (RMS) wavefront error of 3.65 nm and a 0.99997 Strehl ratio for 4-μm light ^[ Reference Cheetham, Tuthill, Sivaramakrishnan and Lloyd ^{116 ]}. In an experimental demonstration, Cheetham et al. ^[ Reference Cheetham, Cvetojevic, Norris, Sivaramakrishnan and Tuthill ^{117 ]} co-phased 18 mirror segments to an RMS wavefront error of 25 nm and a Strehl ratio of 94%. These co-phasing procedures are considered in the active optics class and not the adaptive optics class, meaning they cannot quickly respond to misalignments. An error analysis on the tip, tilt and piston of the tiled parabolic mirror arrangement has been performed to better understand the sensitivity for ultra-high-intensity focusing.

Any random source of error will have a normal distribution. To simulate this, we generate a list of 36 different alignment errors from a Gaussian distribution, centered at zero, with a set error standard deviation. For the piston error this was done using a mirror displacement value, while for tip and tilt an angular error was used. Each of the 36 mirror segments is assigned a value from the error distribution in the ray trace model and the focused intensity is calculated. An example of an error distribution for a piston error with a standard deviation of 40 nm is shown in Figure 19(b). Each standard deviation value is repeated 10 times (i.e., 10 different actuator error lists per standard deviation) in the ray trace code, recording the peak-focused intensity each time, to account for the statistical nature of the error. Figure 19(a) shows the reduction in focused intensity with increasing piston error distribution standard deviation. A standard deviation of 40 nm, with an average RMS error of 38.1 nm, resulted in an average focused intensity error of 5%.

Figure 19

(a) Piston error effect on focused intensity. Error bars represent the standard deviation of the focused intensity for the 10 runs at a particular piston error standard deviation distribution. (b) Example of a randomly distributed piston actuator error for the 36 mirror segments with a 40-nm standard deviation.

The tip–tilt error was analyzed using a similar method, except an angular error of the order of μrad was used. Here, the tip corresponds to rotation about the x-axis of the mirror (i.e., the longer dimension of the mirror is rotated) while the tilt corresponds to rotation about the y-axis of the mirror (i.e., the shorter dimension of the mirror was rotated). The effect of tip–tilt error on focused intensity is shown in Figure 20. For the tip error, an error standard deviation distribution of 0.4 μrad resulted in a 5% decrease in peak-focused intensity, while for the tilt error this was 0.9 μrad. The difference between the two is due to the f-number difference for the different mirror axes. However, if the pointing error is caused by actuator displacements this result should be the same for the two axes since the actuator displacement for the horizontal tilt will produce twice the angular deviation of the tip due to the length difference to the pivot point.

Figure 20

Tip–tilt error effect on the focused intensity. Error bars represent the standard deviation of the focused intensity for the 10 runs at a particular tip or tilt error standard deviation distribution.